Physics
Scientific paper
Jun 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.303..683h&link_type=abstract
Nature (ISSN 0028-0836), vol. 303, June 23, 1983, p. 683, 684.
Physics
9
Neutron Stars, Pulsars, Stellar Structure, Equations Of State, Stellar Evolution, Stellar Rotation
Scientific paper
The recently discovered millisecond pulsar (PSR 1937+214) has been observed to be rotating close to the limit of dynamic instability for a neutron star. In spite of its extremely rapid rotation, the present measurements of the period derivative put a stringent upper limit on the energy loss from gravitational radiation, thus requiring that the quadrupole moment be quite small. The pulsar must also be rotating below the critical frequency at which its equilibrium configuration would become non-axisymmetric, since the lifetime of this configuration against decay by gravitational radiation is very short. This critical frequency imposes a more severe restriction on the rotation rate than the break-up frequency and may be used to set a lower limit, >ρ< > 2×1014 g cm-3, on the density of the star. If the mass is 0.5-1.5 M_sun;, several of the stiffer neutron star equations of state may be ruled out, and the radius should be <16 km.
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